论文标题
$ z = 4 $的超红色超质量星系集群核心的出现
Emergence of an Ultra-Red Ultra-Massive Galaxy Cluster Core at $z=4$
论文作者
论文摘要
对大规模星系群集演化的最新模拟和观察预测，在群集病毒之前，大多数恒星质量积累发生在群集成员中的$ z = 2 $。在$ z> 3 $上富含尘土飞扬的星系星系（DSFG）的原始群体是这些大型星系簇的最受欢迎的候选祖先，价格为$ z \ sim0 $。我们在这里提出了第一项研究，分析了恒星排放以及在光谱镜确认的$ z = 4.002 $ protoCluster核心富含DSFG的稳定的$ z = 4.002 $ tsfg，遥远的红色核心（DRC）中。我们将新的HST和Spitzer数据与现有的Gemini，Herschel和Alma观察结果相结合，以得出单个星系级的特性，并将它们与同时场和其他原始星系进行比较。所有的原始成员都是巨大的（$> 10^{10} $ m $ _ \ odot $），但并不明显比他们的coeval field对应物更重要。在不确定性之内，所有这些都与星形与恒星质量主序列关系以及星形形成效率平面上的星系几乎没有区别。假设没有未来的新鲜天然气涌入，我们估计这些气态DSFG会以$ \ sim300 $ MYR耗尽其气体储层，成为巨大的静态椭圆形占主导地位的群集核心的质量。使用各种方法，我们得出总计$ z = 4 $ halo质量为$ \ sim10^{14} $ m $ $ _ \ odot $，并且估计DRC将演变为成为质量$ $ \ gtrsim10^{15} $ m $ m $ m $ _ $ _ \ odot $ by z x $ z = 0 $的超大群集核心。
Recent simulations and observations of massive galaxy cluster evolution predict that the majority of stellar mass build up happens within cluster members by $z=2$, before cluster virialization. Protoclusters rich with dusty, star-forming galaxies (DSFGs) at $z>3$ are the favored candidate progenitors for these massive galaxy clusters at $z\sim0$. We present here the first study analyzing stellar emission along with cold dust and gas continuum emission in a spectroscopically confirmed $z=4.002$ protocluster core rich with DSFGs, the Distant Red Core (DRC). We combine new HST and Spitzer data with existing Gemini, Herschel, and ALMA observations to derive individual galaxy-level properties, and compare them to coeval field and other protocluster galaxies. All of the protocluster members are massive ($>10^{10}$ M$_\odot$), but not significantly more so than their coeval field counterparts. Within uncertainty, all are nearly indistinguishable from galaxies on the star-forming vs. stellar mass main-sequence relationship, and on the star formation efficiency plane. Assuming no future major influx of fresh gas, we estimate that these gaseous DSFGs will deplete their gas reservoirs in $\sim300$ Myr, becoming the massive quiescent ellipticals dominating cluster cores by $z\sim3$. Using various methodologies, we derive a total $z=4$ halo mass of $\sim10^{14}$ M$_\odot$, and estimate that the DRC will evolve to become an ultra-massive cluster core of mass $\gtrsim10^{15}$ M$_\odot$ by $z=0$.
